OBSERVED BINARY FRACTION SETS LIMITS ON THE EXTENT OF COLLISIONAL GRINDING IN THE KUIPER BELT

@article{Nesvorn2011OBSERVEDBF,
  title={OBSERVED BINARY FRACTION SETS LIMITS ON THE EXTENT OF COLLISIONAL GRINDING IN THE KUIPER BELT},
  author={David Nesvorn{\'y} and David Vokrouhlick{\'y} and William F. Bottke and Keith S. Noll and Harold F. Levison},
  journal={The Astronomical Journal},
  year={2011},
  volume={141}
}
The size distribution in the cold classical Kuiper Belt (KB) can be approximated by two idealized power laws: one with steep slope for radii R > R* and one with shallow slope for R < R*, where R* ∼ 25–50 km. Previous works suggested that the size frequency distribution (SFD) rollover at R* can be the result of extensive collisional grinding in the KB that led to the catastrophic disruption of most bodies with R < R*. Here, we use a new code to test the effect of collisions in the KB. We find… 

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References

SHOWING 1-10 OF 59 REFERENCES

THE COLLISIONAL DIVOT IN THE KUIPER BELT SIZE DISTRIBUTION

This paper presents the results of collisional evolution calculations for the Kuiper Belt starting from an initial size distribution similar to that produced by accretion simulations of that region—a

FORMATION OF KUIPER BELT BINARIES BY GRAVITATIONAL COLLAPSE

A large fraction of ∼100 km class low-inclination objects in the classical Kuiper Belt (KB) are binaries with comparable masses and a wide separation of components. A favored model for their

Formation of Kuiper-belt binaries by dynamical friction and three-body encounters

TLDR
It is shown that a transient binary forms when two large bodies penetrate one another's Hill sphere (the region where their mutual forces are larger than the tidal force of the Sun) and the loss of energy needed to stabilize the binary orbit can occur through dynamical friction from surrounding small bodies, or through the gravitational scattering of a third large body.

The formation of Kuiper-belt binaries through exchange reactions

TLDR
The only required assumption is that the TNOs were initially formed through gravitational instabilities in the protoplanetary dust disk, and the basis of the mechanism is an exchange reaction in which a binary whose primary component is much more massive than the secondary interacts with a third body, whose mass is comparable to that of the primary.

KBO binaries: how numerous were they?

Accretion in the Edgeworth-Kuiper Belt: Forming 100-1000 KM Radius Bodies at 30 AU and Beyond.

We employ a time-dependent collisional evolution code to study the conditions under which the 50{200 km radius Edgeworth-Kuiper Objects (EKOs) in the region between 30 and 50 AU (now called the

Formation of Kuiper-belt binaries through multiple chaotic scattering encounters with low-mass intruders

The discovery that many trans-Neptunian objects exist in pairs, or binaries, is proving invaluable for shedding light on the formation, evolution and structure of the outer Solar system. Based on

Collisional Evolution of Edgeworth–Kuiper Belt Objects

The Edgeworth–Kuiper Belt contains a population of objects ≈103times that of the main asteroid belt, spread over a volume ≈103larger and with relative speeds ≈10 times lower. As for the asteroids,

VELOCITY-DEPENDENT CATASTROPHIC DISRUPTION CRITERIA FOR PLANETESIMALS

The resistance of planetesimals to collisional erosion changes dramatically during planet formation. The transition between accretion and erosion from a collision is defined by the relationship

From the Kuiper Belt to Jupiter-Family Comets: The Spatial Distribution of Ecliptic Comets☆

Abstract We present numerical orbital integrations of thousands of massless particles as they evolve from Neptune-encountering orbits in the Kuiper belt for up to 1 Gyr or until they either impact a
...